[Previous] | [Session 56] | [Next]
D.G. Georgobiani (Michigan State U.), R. Nigam, A.G. Kosovichev (Stanford U.), R.F. Stein (Michigan State U.), A. Nordlund (Teoretisk Astrofysik Center)
In order to study spectral characteristics of the solar oscillations, we use the Stein-Nordlund 3d hydrodynamic code to generate lond temporal sequencies of realistically simulated upper layers of the solar convective zone. The simulation domain ranges from 0.5 Mm above the surface of \tau=1 to 2.5 Mm below this surface, and is 6 Mm by 6 Mm wide. We have generated 24 hours of solar time.
We calculate power spectra of the vertical velocity and temperature at different heights and the emergent intensity at the surface. Here, we present the profiles of velocity, intensity and temperature for both radial (\ell = 0) and first nonradial (\ell = 700) mode.
We compare line profiles from the simulation with the power spectra of the Doppler velocity and continuum intensity from the SOHO/MDI observations. Both simulated and observed profiles demonstrate similar types of asymmetry, and the asymmetry reversal between the local quantities like velocity and temperature, and emergent intensity profiles is also present in the simulated data.
The preliminary results are promising as they allow us to establish a connection between the observational data and realistic simulations, and enable us to understand better the physics of solar oscillations.
If the author provided an email address or URL for general inquiries, it is a
s follows: